Meteorites formed under highly reducing conditions can incorporate substantial amounts of Si in solid solution in their metallic phases. In enstatite meteorites, reduced Si appears in shreibersite, perryite and, in variable amounts, in the kamacite, taenite, and tetrataenite. Microprobe bulk analysis of Si in Fe,Ni particles of aubrites show a large variation from grain to grain; this large compositional range has been attributed to local equilibrium conditions in the specific T and/or fO2 environments in which they are formed. Si concentrations are homogeneous in the kamacite; in contrast, the Ni-rich phases (taenite and tetrataenite) show a characteristic Si profile. Concentrations of this element in tetrataenite are substantially higher than in the adjacent kamacite, and decrease smoothly towards the center of the taenite grain, matching very closely the M-shaped profile of Ni. Other elements with similar distribution patterns are Ge and Cu. A satisfactory explanation for this behavior cannot be given in the absence of experimental data for the diffusion of Si between alpha and gamma-Fe alloys. However, two end-member possibilities can be envisioned: the distribution of Si between kamacite and taenite may be controlled by (1) the crystallographic structure or (2) the chemical composition of the host phases. These possibilities are explored.